Hot jupiters are uncommon, but not rare, however I don't know how many known ones would count as evaporating. They (evaporating planets that is, not just hot jupiters) would be more common around hotter stars of course.

The diamond planet at 55 Cancri and the recently discovered Alpha Centauri planet would count as well.

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Can planets with highly elliptical orbits dynamically be evaporating or not, depending on distance?

Considering his answer to a question of mine that is asking the same kind of thing, I would guess yes.

I'm curious to see what the dynamics would be in multiple star systems with widely separated orbits since such comets would be thrown all over the place.

That planet that I found colliding with one of it's stars would look awesome in a timelapse as it approached it's doom.

Many comets' tails are a hundred million kilometers long or more, and their comas can be over a million kilometers across. So it seems realistic to me. My only point would be that the ion tails on some of those comets look just a little too bright. But it's a minor observation.

Yea the comets look fine to me. The second planets tail seems rather spread out (compared to the third planet), but there could be various things contributing to that such as the planets size and any moons that it has could be adding to the spread of it.

I'm not saying that it looks implausible since a comet could have a wide tail like that, but I'm not sure what would be making it do that.

I suppose the logical answer would be that the tail would go in the combined opposite direction of the two stars, or if the object is closer to one star than another, have the direction be mainly dictated by the closer star.

I know SE is set to have planets be no closer than it would reach 2000k at any point (highly elliptical orbits and binaries can create exceptions to this), but it would be cool to allow a certain percentage of the comets come very close to their primary star (or stars).

Also, will there be a melted surface subtype for each procedural model of rocky planet (or at least the ones that would exist in the inner system)?

After two days, I'm recovering my ability to communicate, so I can make some notes on the new feature. Well, I asked about that for about a 8 month ago, although I never expected something like evaporating planet tails.

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But I think the tails are too much big, don't you think?

Seems that it is not that the tails are too big, but they're too bright, probably, a luminosity needs to be tweaked.

Quote (Salvo) There are Chthonian planets on Space Engine? Because an evaporating planet will become a Chtonian planet someday I do not believe so, I hope Space Engineer adds them with maybe some other planet classes

We don't have those yet, but this is definetly a stepping stone towards adding them.

While I know that this planet either wouldn't exist, or if it did, it would be glowing hot and molten anyway, whether that planet should exist as formed yet* isn't my question. My hypothetical question is that with the new 'melted surface' planets at a temperature of 2000k+ (or 1500+? or whatever you set the temperature mark as for the surface melting), how would that be applied to asteroids and selenas?

*Space Engineer, you talked about planetary formation on another thread (or maybe it was the work in progress thread) and had said about limiting planet formation for very short lived stars or something, are you still doing that? Those aren't your exact words, but it was during a discussion about short lived stars and planet formation.